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G. D. Holman (NASA/GSFC), J. T. Mariska (NRL), J. M. McTiernan (UC Berkeley), L. Ofman (Raytheon ITSS), V. Petrosian (Stanford U.), R. R. Ramaty (NASA/GSFC)
HESSI, the High Energy Solar Spectroscopic Imager, will observe the x-ray and gamma-ray emission from solar flares with an unprecedented combination of spectral, spatial, and temporal resolution. The quantitative interpretation of the HESSI data will require a level of numerical modeling not generally demanded by previous observations. In view of this, we are developing an integrated package of modular numeric codes and models for the analysis and interpretation of these data. The package will focus on the energetic electrons produced during the impulsive phase of flares. It will compute both the bremsstrahlung x-ray/gamma-ray emission and the gyrosynchrotron radio emission from model flare configurations and initial electron distributions. Steady-state and time-dependent Fokker-Planck codes will compute the transport of suprathermal electrons. A hydrodynamic code will compute the response of the flare plasma in the model configurations. The proposed computational package will allow for comprehensive modeling of energized electrons in different flare scenarios. The predicted emissions can be compared directly with HESSI and radio images and spectra. The package will provide the necessary framework for comparing electron acceleration models with HESSI data.
This work is supported in part by the NASA Sun-Earth Connection Program.
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